J/A+A/619/A166 SEDIGISM, kinematics of ATLASGAL filaments (Mattern+, 2018)
SEDIGISM: the kinematics of ATLASGAL filaments.
Mattern M., Kauffmann J., Csengeri T., Urquhart J.S., Leurini S.,
Wyrowski F., Giannetti A., Barnes P.J.,Beuther H., Bronfman L.,
Duarte-Cabral A., Henning T., Kainulainen J., Menten K.M., Schisano E.,
Schuller F.
<Astron. Astrophys. 619, A166 (2018)>
=2018A&A...619A.166M 2018A&A...619A.166M (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Molecular clouds ; Carbon monoxide
Keywords: molecular data - methods: data analysis - stars: formation -
ISM: clouds - ISM: kinematics and dynamics - submillimeter: ISM
Abstract:
Analyzing the kinematics of filamentary molecular clouds is a crucial
step toward understanding their role in the star formation process.
Therefore, we study the kinematics of 283 filament candidates in the
inner Galaxy, that were previously identified in the ATLASGAL dust
continuum data. The 13CO(2-1) and C18O(2-1) data of the SEDIGISM
survey (Structure, Excitation, and Dynamics of the Inner Galactic
Inter Stellar Medium) allows us to analyze the kinematics of these
targets and to determine their physical properties at a resolution of
30-arcsec and 0.25km/s. To do so, we developed an automated algorithm
to identify all velocity components along the line-of-sight correlated
with the ATLASGAL dust emission, and derive size, mass, and kinematic
properties for all velocity components. We find two-third of the
filament candidates are coherent structures in
position-position-velocity space. The remaining candidates appear to
be the result of a superposition of two or three filamentary
structures along the line-of-sight. At the resolution of the data, on
average the filaments are in agreement with Plummer-like radial
density profiles with a power-law exponent of p~=1.5±0.5, indicating
that they are typically embedded in a molecular cloud and do not have
a well-defined outer radius. Also, we find a correlation between the
observed mass per unit length and the velocity dispersion of the
filament of m∝σv2. We show that this relation can be
explained by a virial balance between self-gravity and pressure.
Another possible explanation could be radial collapse of the filament,
where we can exclude infall motions close to the free-fall velocity.
Description:
In this study we studied spectral line emission from 283 filament
candidates detected with ATLASGAL continuum dust emission from the
catalog of Li et al. (2016, Cat. J/A+A/591/A5) in the SEDIGISM 13CO
and C18O survey.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table56.dat 188 422 Measured and derived parameters
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See also:
J/A+A/591/A5 : ATLASGAL dense filamentary structures (Li+, 2016)
Byte-by-byte Description of file: table56.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- ID Filament ID, GLLL.lll+BB.bbb_N (fil_id)
19- 24 F6.2 deg GLON Galactic longitude of the center of the
filament (gal_long)
26- 30 F5.2 deg GLAT Galactic latitude of the center of the
filament (gal_lat)
32- 51 A20 --- Status Correlation with the ATLASGAL emission
(status)
53 I1 --- Ncomp Number of detected velocity components in
the original filament candidate (n_comp)
55- 61 F7.2 km/s v13CO Peak velocity derived from the 13CO
average spectrum (velocity_13CO)
63- 69 F7.2 km/s vC18O ?=- Peak velocity from the C18O average
spectrum (velocity_C18O)
71- 74 F4.2 km/s s_v13CO Dispersion of the 13CO peak velocities
along the skeleton (sigpeak13CO)
76- 80 F5.2 km/s s_vC18O Dispersion of the C18O peak velocities
along the skeleton (sigpeakC18O)
82- 85 F4.2 km/s sigma Average total velocity dispersion along the
skeleton (derived from 13CO and C18O)
(sigma)
87- 90 F4.2 km/s sigma13CO Average 13CO velocity dispersion along the
skeleton (sigma_13CO)
92- 97 F6.2 km/s sigmaC18O ?=- Average C18O velocity dispersion along
the skeleton (sigma_C18O)
99-102 F4.2 km/s <sigma13CO> 13CO velocity dispersion derived from the
average spectrum (sigaver13CO)
104-109 F6.2 km/s <sigmaC18O> ?=- C18O velocity dispersion derived from
the average spectrum (sigaverC18O)
111-115 F5.1 kpc Dist ?=- Distance from the Sun (distance)
117-122 F6.2 pc Length ?=- Physical length of the detected
skeleton (length)
124-127 F4.2 deg LengthAng Angular length of the detected skeleton
(angular_length)
129-135 F7.1 Msun Mdustatg ?=- Filament mass derived from ATLASGAL
emission (Mdustatg)
137-144 F8.1 Msun Mdustatp ?=- Filament mass derived from
ATLASGAL+PLANCK emission (Mdustatp)
146-153 F8.1 Msun Mdustatpc ?=- Filament mass derived from corrected
ATLASGAL+PLANCK emission (Mdustatpc)
155-162 F8.1 Msun Mgas ?=- Filament mass derived from integrated
13CO emission (M_gas)
164-169 F6.1 Msun/pc mobs ?=- Observed line-mass (m_obs)
171-174 I4 Msun/pc mvir Critical, non-thermal line-mass (m_vir)
176-179 F4.2 --- d13CO Fraction of the skeleton detected in 13CO
(detection_13CO)
181-184 F4.2 --- dC18O Fraction of the skeleton detected in C18O
(detection_C18O)
186 I1 --- FlagEdge [0/1] Skeleton truncated because of the
edge of SEDIGISM (edge_flag)
188 I1 --- f_Dist [0/2] indicating the method for the distance
estimate (dist_flag) (1)
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Note (1): Flag for method for the distance estimate as follows:
0 = no distance;
1 = inside ATLASGAL source
2 = nearby ATLASGAL source
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Acknowledgements:
Michael Mattern, mmattern(at)mpifr-bonn.mpg.de
(End) Michael Mattern [MPIfR, Germany], Patricia Vannier [CDS] 24-Oct-2018